V.G. KurtV.G. Kurt11, V.V. Sokolov, V.V. Sokolov22, V.N. Komarova, V.N. Komarova22, , Yu. A. ShibanovYu. A. Shibanov33

““Optical observations radio Optical observations radio pulsars and isolated neutron pulsars and isolated neutron stars with 6 meters telescope stars with 6 meters telescope

BTA SAO RANBTA SAO RAN””1 1 Astro Space Center of the P.N.Lebedev Physical Inst. Astro Space Center of the P.N.Lebedev Physical Inst. of the Russian Academy of Sciences, Moscow, Russiaof the Russian Academy of Sciences, Moscow, Russia

vkurt@asc.rssi.ruvkurt@asc.rssi.ru2 2 Special Astrophysical Observatory of the Russian Special Astrophysical Observatory of the Russian Academy of Sciences, Nigniy Arkhiz, Karachavo-Academy of Sciences, Nigniy Arkhiz, Karachavo-

CherkessiaCherkessia, , RussiaRussia

3 3 S-Petersburgh Physical – Technical Institute S-Petersburgh Physical – Technical Institute name name

A.F. Ioffe, Russia A.F. Ioffe, Russia

Location SAO RANLocation SAO RAN

6 meter optical telescope BTA6 meter optical telescope BTA1966 y1966 y

Winter viewWinter view

6 m telescope BTA inside6 m telescope BTA inside

Optical schemaOptical schema

Optical corrector SCORPIO in main Optical corrector SCORPIO in main focusfocus

The main parametersThe main parameters• The main mirror is parabolic shape focal length is

24 m. The diameter of the main mirror is 605 cm. In prime focus cage, where optical devices and the mechanisms of input/output of the lens corrector and hyperbolic secondary focus mirror are located. From the laboratory tests the concentration of energy in a circle 0.8" in diameter is 90%. Under favorable conditions the seeing is limited by atmosphere amounts to FWHM ~1" for 20% of observational nights and 1.8’’ tipical.

• The optical scheme of the telescope provides for working at the prime focus (f/4) and two Nasmith foci (f/30). To correct for field aberrations, when working at the prime focus, a Rosse corrector is used, which is made of K type glass (the short-wave bandwidth is 3800A ). The field of view with coma and astigmatism corrected at a level of <0.5" is about 14'.

Some parameters of BTA TelescopeSome parameters of BTA Telescope• The 6-m telescope (BTA - Big Telescope Alt-

azimuthal) The telescope is located near Mt. Pastukhova at an altitude of 2070 m above sea level, the coordinates of the site: longitude N 41o26'30", latitude E +43o 39'12".

• Main mirror diameter 6 m. Focal length 24 m. Light collecting area 26 sq.m Wavelength range 0.3 - 10 mkm. Angular resolution 0.6 arcsec- with the application of speckle interferometry techniques 0.02 arcsec. Mass of the main mirror 42 tons Total telescope mass 850 tons. Telescope Dome is D= 42 m, H = 53 m, Limiting stellar magnitude near 26m for V, R, I (system)

DETECTORSDETECTORS• CCD - photometer

• The Prime Focus CCD-photometer• of 1024 x 1024 pixels cooled with liquid nitrogen to a temperature of

-120oC The optical and mechanical design of the photometer contains a weal with 12 filters, a fast section shutter and standard lamp for flat-field calibrating. The size of the registered field of view of the photometer in PF BTA is 210.3" x 210.3", the pixel size is 24x24mkm which correspoded angular size in PF BTA 0.205"x0.205". Readout noise is 2.85e – per sec .

• The set of wide-band filters used in photometry is system similar to the Jonson and Cousins B V R I. A set of narrow-band filters in the region of Hα line for the observations of galaxies in the range the redshifts z = 0.000 - 0.033 is available. Soft - MIDAS from ESO.

• Band BVRI extinction coefficient 0.340; 0.210; 0150; 0.100m

Limiting mag Texp = 600s and S/N=4 26.1m 25.6m 25.1m 24.4m Sky brightness 22.5 21.5 20.8 19.1 m / sq.sec

NEWNEW

• New CCD EEV 42-40 with 2048x2048 pixels (equals 6.1' on sky). New

photometric soft - instead of MIDAS, now we use IRAF ( Image Reduction and Analysis Facility). For astrometry our soft is IRAF.

 

OUR PHOTOMETRYOUR PHOTOMETRY

• log f = - 0.4 mx + log f (0) erg cm-2 s-1A-1

For V logf (0) = - 8.440• R - 8.760• I - 9.080• J -9.497• K -10.380• Typical seeing ………………………1.3 - 1.8 ” (!)• VERY BAD! For HST S/N=50 BTA ~ 7• 10 – 20 weak stars for calibration in field near 30”

Catalog of radio pulsarsCatalog of radio pulsars

• http://www.atnf.csiro.au/research/pulsaat/ 1794 Radio pulsars with Δα and Δδ 0.1 – 0.001 ang. sec (except VLBI measurements near 1%).

• This is our hard astrometry problem! “Step to step movements “

PSR 0656+14PSR 0656+14

Search of pulsarsSearch of pulsars• F =4 r2 T4 /4 d2 (erg cm-2 s-1 )

• Low Interstellar absorptions, |b| > 5-10o

• To = T /106 , K

• Ro = r /10 km

• do = d / 500 pc d < 1000 pc

• For T0 =R 0=d 0 = 1 without absorptions

• V = 24m it is good!

• Very Young τ =P/(2 dP/dt) < 10 8 y

X-ray and gamma ray emissionX-ray and gamma ray emissionfor PSR 0656+14for PSR 0656+14

• ROSAT• Soft BB radiation T= 840 000 K• Hard chanall T = 1 650 000 K

• GROPower law = -1.8 (±0.3)

CCD picture for PSR 0656+14CCD picture for PSR 0656+14

Photometry HST and BTAPhotometry HST and BTA

Spectrum of PSR 0656+14Spectrum of PSR 0656+14

Two parameters Two parameters

• 1) Raylegh – Jeans parameter G =T6 ( R10 /d500 )2

2)Energy power-low index By fitting of spectrum 0 < G< 6.2 for 1 level 0.3 < < 2.6 1 level Exist non-thermal component

Gamma-Radio pulsar GEMINGAGamma-Radio pulsar GEMINGA

• Multiband photometry of Geminga• Kurt, V.G.; Komarova, V.N.; Sokolov, V.V.; Fatkhullin, T.A.;• Koptsevich, A.B.; Shibanov, Yu.A.• Bulletin of the Special Astrophysical Observatory Vol. 51, p. 21 - 37

(2001)• Abstract• We present the results of the BVRI photometry of the Geminga pulsar

based on observations with the 6 m telescope. The Geminga magnitudes in B (26.1m+/-0.5), V (25.3m+/-0.3) and Rc (25.4m+/-0.3) are consistent with results of other studies of its optical emission in these spectral bands. We derive for the first time the magnitude in the Ic band to be 25.1m+/-0.4, which is more than a magnitude higher if compared with the upper limit given in the paper of Mignani et al. (1998). The comparison of the broad-band spectra of this middle-aged isolated neutron star with the results of observations in the X-rays and hard ultraviolet suggests non-thermal origin of the Geminga emission at least in some band of the visible range.

OTHER SOURCESOTHER SOURCES

• Optical studies of neutron stars and their surroundings• at the 6m telescope of SAO RAS}• V.N. Komarova, T.A. Fatkhullin, V.G. Kurt, Yu.A. Shibanov• Physics of Neutron Stars-2005

• The results of the on-going program for study of optical counterparts of pulsars and candidates to isolated neutron stars (NS) and search for pulsar wind nebulae (PWNe) in the H line at the 6m telescope SAO RAS are presented. Broad- and narrow-band observations have been carried out with the prime focus photometer and the focal reducer SCORPIO in image mode. There are close and/or high energetic (high velocity) NSs and pulsars, such as RX J0007+7302, AXP 4U0142+61, PSR B0823+26, PSR B1951+32, RBS 1774, PSRB2334+61 and others, in a target list. Upper limits on the level of detection and flux estimates of the objects under investigation have been obtained.

Comparison pulsars with different agesComparison pulsars with different ages

9500A9500A9500A9500 A

3000 A3 mkm

AGE of OUR PulsarsAGE of OUR Pulsars

• Crab 1 103 years

• VELA 1.13 104

• GEMINGA 1.5 103

• B 0656+14 1.1 105

• B 0540 - 69 1.67 103

The The IsolatedIsolated, Radio-Quiet , Radio-Quiet Neutron Star Neutron Star RXJ 185635-3754RXJ 185635-3754

Walter & Lattimer (2002)

Two backbody fit:T1=64 eVT2=30 eVRinf=12-26 km

Pure Hmodel

LITERATURELITERATURE• Bibliography

• for report V. G. Kurt at Conference “Frontiers of Space Astrophysics: Neutron Stars and Gamma Ray Bursts”

• 1). Optical Observations of the Nearby Isolated Pulsar PSR 0656+14 at the SAO 6-meter Telescope.

• Kurt, V. G., Komberg B. V., Sokolov, V. V., Zharykov S. V.• Astrophysics and Space Science, v. 252, Issue 1/2, p. 451-460.• 2). BVRI observations of PSR B0656+14 with the 6-meter telescope• Kurt, V.G., Sokolov V.V., Zharikov S.V., Pavlov G.G., Komberg, B.V.• Astronomy and Astrophysics, v.333, p.547-556 (1998)• 3). Optical Observations of the Nearby Isolated Pulsars With the 6 Meter Telescope• Sokolov V.V., Kurt, V.G., Zharikov S.V., Shibanov Yu.A., Koptsevich A.B.• Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and• Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.: J.Paul, T.Montmerle,• and E. Aubourg (CEA Saclay)• 4). Photometric study of fields of nearby pulsars with the 6m telescope.• Kurt V.G., Komarova V.N., Fatkhullin T.A., Sokolov, V.V.,• Koptsevich A.B., Shibanov Y.A.• Bulletin. Special Astrophys. Obs., 49, 5-13 (2000)• 5). Multiband photometry of Geminga• Kurt, V.G., Komarova V.N., Sokolov V.V., Fatkhullin T.A.,• Koptsevich A.B., Shibanov Yu.A.• Bulletin of the Special Astrophysical Observatory Vol. 51, p. 21 - 37 (2001)

• 6). Optical photometry of the PSR B0656+14 and its neighborhood• Koptsevich A.B., Pavlov G.G., Zharikov S.V., Sokolov, V.V.,• Shibanov Yu.A., Kurt V.G.• Astronomy and Astrophysics, v.370, p.1004-1016 (2001)• 7). "Фотометрические исследования центральной области CTB 80",• В.Н. Комарова, В.Г. Курт, В.В. Соколов, Ю.А. Шибанов,• 2001, Тезисы докладов ВАК-2001, 94• 8). Фотометрические исследования оптического излучения пульсаров• В.Н. Комарова, В.Г. Курт, В.В. Соколов, Ю.А. Шибанов• Всеpоссийская Конфеpенция Астpофизика Высоких Энеpгий Сегодня и Завтpа• HEA-2003• 9). Окрестности пульсара B1951+32 в оптике• В.Н. Комарова, В.Г. Курт, В.В. Соколов, Ю.А. Шибанов• Всеpоссийская Конфеpенция Астpофизика Высоких Энеpгий Сегодня и Завтpа• HEA-2003• 10). Optical studies of neutron stars and their surroundings• at the 6m telescope of SAO RAS}• V.N. Komarova, T.A. Fatkhullin, V.G. Kurt, Yu.A. Shibanov• Physics of Neutron Stars-2005• 11). OPTICAL SEARCH FOR COUNTERPARTS TO ISOLATED NEUTRON STARS

AT THE 6METER TELESCOPE OF SAO RAS• V.N. Komarova, V.G. Kurt, Yu.A. Shibanov• Physics of Neutron Stars-2008

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• We want to find anybody who want to study South Sky !

• Many thanks for your attention!